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First discovery of QPOs in the dwarf nova HS 2325+8205 based on TESS photometry

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arxiv 2302.05887 v1 pith:WQBHQYVN submitted 2023-02-12 astro-ph.SR

First discovery of QPOs in the dwarf nova HS 2325+8205 based on TESS photometry

Qi-Bin Sun , Sheng-Bang Qian , Li-Ying Zhu , Ai-Jun Dong , Qi-Jun Zhi , Wen-Ping Liao , Er-Gang Zhao , Zhong-Tao Han
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Wei Liu Lei Zang Fu-Xing Li Xiang-Dong Shi
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classification astro-ph.SR
keywords orbitalqposdwarfintensitynovaoscillationperiodfind
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HS 2325+8205 is a long-period eclipsing dwarf nova with an orbital period above the period gap (Porb>3 h) and is reported to be a Z Cam-type dwarf nova. Based on the photometry of the Transiting Exoplanet Survey Satellite (TESS), the light variation and the quasi-periodic oscillation (QPOs) of HS 2325+8205 are studied. Using Continuous Wavelet Transform (CWT), Lomb-Scargle Periodogram (LSP), and sine fitting methods, we find for the first time that there is a QPOs of ~ 2160s in the long outburst top light curves of HS 2325+8205. Moreover, we find that the oscillation intensity of the QPOs of HS 2325+8205 is related to the orbital phase, and the intensity in orbital phases 0.5-0.9 are stronger than in orbital phases 0.1-0.5. Therefore, the relationship between the oscillation intensity of QPOs and the orbital phase may become a research window for the origin of QPOs. In addition, we use the LSP to correct the orbital period of HS 2325+8205 as 0.19433475(6) d.

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